This years MEGA 10 Most Beautiful is the celebration of beauty deep within beauty. Its the beauty that everyone can appreciate, not just the physical beauty but the beauty in excellence in every way a true woman should be. In talent, in influence and in existence.
Co-presented by Watson's and L'Oreal Paris, MEGA toasted this year's 10 Most Beautiful women at Republiq Super Club. Led by the magazine's 2014 May cover girl actress Andi Eigenmann, the theme was unconventional pretty. Others who made the list were singer Radha Tinsay, Asia's Next Top Model Cycle 2 finalists Jodilly Pendre and Katarina Rodriguez; actress Mercedes Cabral, photographer Shaira Luna, designer Charina Sarte, singer Abby Asistio, model Sanya Smith, and multi-hyphenate Martine Cajucom. As Republiq filled to near capacity, the program started Watson's Hair Affiar Show, featuring the works of some of the country's top hair stylists: duo Jude Hippolito and Rose Velasco, Karina Mantolino, Louis Phillip Kee, and Nikki Bacay.
how about the taken Tiff and the single Jessa?
Hanging Knit Single Kacci and over-print complicated Jen!
DJ Yoshi came on the decks and sums up the night! people started dancing like everyone was watching. After all, it didn't matter if you wore black or white or didn't fit the mold—it was night to celebrate beauty, in all shape and form.
MEGA Magazine's 10 Most Beautiful would like to thank its co-presentors Watsons and L'Oreal Paris; major sponsors Metro Dental and Bio Oil as well as Figlia an Ysabel's Daughter.
The fight was a tough one, winning over 2 Filipinas (Jodilly and Katarina), Malaysian Model Sheena is the winner of this years cycle 2 of Asia's Next Top Model!
Garage Young Talents turns 5!
GARAGE held the 5th anniversary of its Young Talents roster in SKYE last March 6. The event was attended by the hottest and most stylish denizens in the metro who bore witness to the naming of this year's to-watch-out-for list. And to cap the evening's festivities, attendees were treated to the reunion of the men's style magazine's most successful past Young Talents winners.
Besides being an indispensable source for men's style and grooming, GARAGE is also known to keep abreast with emerging talents in different creative fields spanning fashion, entertainment, design, culture and the arts. It was due to this hotbed of talent that the Young Talents roster of the magazine was created. GARAGE, being a creative force in the fashion industry in itself, nurtures the same spirit in others by turning the spotlight on these individuals whose talents have made an impact in their respective fields. The magazine has been celebrating this creative force for the past five years since its inception. Past winners have included Enchong Dee, Sam Concepcion, Chris Cayzer and more.
The evening began with a fashion show directed by Robby Carmona and sponsored by clothing brand, Folded and Hung. It was then followed by the announcement of this year's Young Talents list which includes athlete Andre Paras, make-up artist Nikki Duque, stage actor Rafa Siguion Reyna, artist Mano Gonzales, model LA Aguinaldo, designer Lorenz Namalata, muse Janna Tee and writer Margarita Buenaventura. But the highlight of the GARAGE Young Talents 5th Anniversary celebration was the reunion of the past year's winners which included Enrique Gil, Alden Richards and Elmo Magalona who are incidentally, also the cover stars of the February 2014 issue of GARAGE.
The theme of the evening was PARADISE SWING and guests were seen in their modern tropical looks reminiscent of 40's Hawaii, Pearl Harbor and From Here to Eternity. The February issue of GARAGE saw cover stars Enrique Gil, Alden Richards and Elmo Magalona interpreting this theme by donning a special collection featuring a collaboration of brand, Folded and Hung with hot designer, Bang Pineda. The current issue is dubbed as a special magazine because it features not only the current roster of Young Talents but all the past winners as well.
The GARAGE Young Talents 5th Anniversary event is sponsored by Folded and Hung, Blackwater Scents, Skye, Saga Events and official drink sponsor, Hennessy.
The February 2014 issue of GARAGE featuring the current and past roster of Young Talents is currently available in all major bookstores, newsstands, department stores, supermarkets and convenience stores for the regular price of P150. Hurry! Grab a copy today!
GARAGE magazine is the modern guy's guide to style. It features the latest news and trends in men's style and grooming and inspires its readers to create their own individual style. GARAGE is known for its experimental approaches in magazine format and printing and is acknowledged for its world-class fashion editorials. GARAGE remains to be the only men's fashion magazine in the country today.
When I first saw the collection of Jairus Sumineg from his past works till our first collaboration last 2012, I bet that this young designer from Baguio got really the eye for fashion, and with his talent he just need to be seen and be recognized.
Raw, Innovative and Avant garde, when I saw his latest collection Chimera, its so L-O-V-E. I'm so honored when he said that I will shoot Chimera.
Check out the looks of Baguio's Top Designer Jairus Sumineg in Hermitism by Herminio Tan Accessories.
Jewelmer Joaillerie will welcome luminaries, leaders, and friends at the second annual Jewelmer Gala held on October 15, 2013 at the NBC Tent for the launch of its Spring/Summer Collection 2014.
"Playing with the sensuality of the five senses, we reveal the creation of our collections with the rarest pearls on earth," says Director Jacques Christophe Branellec. While they have already made their international debuts in Hong Kong and Moscow, the Charleston, Guimard, Madame de Pompadour, C'est la Vie collections will be formally launched on this evening. Together with sumptuously expanded Tropics, Rosone, Petite Fleur, Dolce Rosa, and Via Rosa, they comprise Jewelmer Joaillerie's Spring/Summer Collection 2014.
Inspired by the nine collections by Jewelmer Joaillerie come the creations of to designers including including Rhett Eala, Patrice Ramos Diaz, Randy Ortiz, Ivarluski Aseron, JC Buendia, Francis Libiran, Albert Andrada, Jojie Lloren, and Jun Escario. Every tableau, directed by Saga's Robby Carmona, will unfold seamlessly to convey each collection's essence by captivating audiences with a rich journey through the senses.
The purveyor of fine South Sea pearls also celebrates the success of the world's first jewelry co-branded MasterCard with the Jewelmer Joaillerie Platinum Mastercard powered by PNB Allied Bank. Clients can expect curated benefits and premium services for to fit their lifestyles. Moet Hennessy comes in once again to ensure that every glass is full of Belvedere and Grand Marnier while a gourmet spread by Margarita Fores will await guests after the show.
Jewelmer is an international luxury brand that was born out of a commitment to the world's most lustrous South Sea pearls and exquisite fine jewelry that showcases the creative harmony of French design and Asian sensibilities. Established in 1979 by a French pearl farmer and a Filipino entrepreneur, Jewelmer has grown globally to represent a world of rarity and enduring elegance.


They investigated the coaching education and academic background of high performance team coaches. The coaches completed an online questionnaire before undertaking a semi-structured qualitative interview. The results show that formal education courses are not meeting the demands of high performance coaches, who prefer to learn from more informal settings, relying on self-directed learning and coaching experience to continue to develop. More research is needed to examine how this learning is applied in practice.


In international development circles, the application of machine learning to monitor and alleviate poverty interventions has become a much discussed aspiration. However, Joshua Blumenstock, assistant professor at the UC Berkeley School of Information and director of the Data-Intensive Development Lab, cautioned at a recent Blum Center Faculty Salon that unknowns abound and new digital methods may serve more as a complement than a replacement to traditional approaches, especially in the area of economic assessment.
At the salon, Blumenstock highlighted two ways big data is altering the field of international development: first, in measuring quality of life and welfare in low-income countries; and second, in offering financial inclusion applications for poor populations. His colleague Moritz Hardt, assistant professor of electrical engineering and computer science, provided a lead response, drawing from his decade of research on fairness and machine learning. Together, they highlighted that over the past five years big data sets—from mobile phone companies, satellite imagery, social media platforms, and international development organizations—paired with advances in machine learning technology, have generated fascinating and controversial work.
A key contributor to these new data sets is the stunning rise in cell phone adoption. According to the World Bank, more households in developing countries own a mobile phone than have access to electricity or clean water, and nearly 70 percent of the bottom fifth of the population in developing countries owns a mobile phone (note: not a smartphone). An increase in satellite and remote sensing data has also contributed to the data explosion. The combination of these data sources, with machine learning, means that data can be synthesized and applied in new ways.
Blumenstock said that satellite imagery in particular is becoming a key source for development research because it reveals basic physical infrastructure and quality of life trends, such as roof material, road quality, and land plot size. This information can help researchers estimate the basic traits of a town, including average household wealth and population density. Blumenstock is currently conducting research with Facebook to provide a publicly available map of micro-regional estimates of wealth and poverty.
"Leveraging machine learning to analyze these forms of data, we can draw conclusions about certain aspects of quality of life with nearly the same accuracy as traditional, multi-million dollar field surveys," Blumenstock explained.
Given the time and cost savings, international multilateral organizations like the World Bank and United Nations are eager to start applying these big data applications. Likewise, many governments in developing countries are eager to bypass traditional data collection methods in favor of machine learning-assisted data analysis because of the large time and monetary costs of national census surveys.
Blumenstock is hopeful that by supplementing traditional poverty indices with high-frequency estimates based on satellite and digital data, development practitioners can have low-cost options for impact evaluations and project monitoring. He said this data-plus-machine-learning approach could help open up major innovations in three areas: 1) targeting specific populations for program implementation; 2) monitoring and mitigating the effects of natural disasters, health epidemics, and migration patterns by allowing, for example, aid workers to deliver needed resources to hard-hit areas; and 3) enabling different approaches to impact evaluation, specifically randomized control trials, which can costs millions of dollars.
Financial inclusion was the other area Blumenstock highlighted as potentially benefiting from algorithm-based decision making. He pointed out that globally 1.7 billion people lack a bank account, half of whom are women in poor, remote regions—yet about two-thirds of this population have access to a mobile phone. Companies like M-Pesa, launched in 2007 in Kenya, are engaged in wide-scale mobile phone-based money transfering, financing, and micro-financing services. As a result, there has been a surge in "digital credit" banking led by the private sector in low-income countries, which is increasing financial inclusion for populations without formal credit.
Using data to analyze phone use patterns, some banks and intermediary financial technology (fintech) companies are testing ways to develop alternative digital credit scores to provide uncollateralized loans to the unbanked. By aggregating digital trace data that includes Internet searches, emails composition, even browser and smartphone choices, and then using machine learning to assess the data, banks can formulate digital credit scores that predict who is most likely to default on a loan. One of the largest entitles to use this approach is a Kenyan digital savings and loan product called M-Shwari, which is built on M-PESA and run by the Commercial Bank of Africa and the mobile network operator Safaricom. Using M-Shwari, customers who lack a bank and credit history can take out loans. Beyond increasing accessibility to loans, digital credit also has the potential to dramatically reduce transaction costs and provide immediate disbursement.
Providing loans to previously unbanked populations can stimulate critical economic growth. Yet Blumenstock was quick to point out that the concept of digital credit scoring and it's rapid growth across developing economies raises several concerns. First, most of these loans are short-term with very high interest rates, which can indebt customers. Second, leaning too heavily on algorithms to churn out credit scores can create a variety of biases.
Blumenstock recently visited Kenya to gain greater insight into the mobile banking process, where digital loans have quickly risen in popularity. According to a 2018 study led by FSD-Kenya, more than one in four Kenyans have taken out a digital loan over the past five years, comprising an estimated 6 million Kenyan borrowers. At the time of the study, more than half of these digital borrowers had at least one outstanding loan, and 14 percent had digital loans from multiple banks. Among the long-term implications to digital credit-based loans are credit bubbles, over-indebtedness, and the overall impact on social welfare.
Lead discussant Moritz Hardt spoke on the limitations of machine learning, particularly in relation to gender and race biases, and their corresponding consequences to everything from credit scores to healthcare predictions to providing child services to decisions in the criminal justice system.
Hardt provided an example of how risk assessment algorithms are used as a predictive tool to determine which individuals are at high risk for missing their court date following an arrest. If deemed as pretrial "high risk" by the algorithm, an arrested individual is held in jail until their court date, with often dire consequences for their income and family circumstances. Such predictive algorithms are similarly used to inform criminal justice officials decisions on how high to set the bail, sentencing, and who gets early release.
"What is often neglected in designing algorithms are the structural and complex socio-cultural challenges unique to each person," Hardt said.
Blumenstock responded that "we need to endogenize social sciences into machine learning," warning that taking off-the-shelf algorithms for ad targeting and plopping them into poverty targeting would have obvious negative results.
Originally published as "Joshua Blumenstock: The Knowns and Unknowns of Big Data and Poverty Alleviation" by the Blum Center for Developing Economies on March 18, 2019.


WWE Crown Jewel happens in 24 hours so we should talk about it all. The card, John Cena, Daniel Bryan, Renee Young, HULK HOGAN! It's all gone mad, which means it's time for a chat. Please do support the podcast at http://www.patreon.com/simonmiller316 and give us 5* on iTunes.


text:
<?php

/* AcmeDemoBundle:Welcome:index.html.twig */
class __TwigTemplate_7100a103999f806301a90ceb19ffd462186d1d31f630125caf97193d304395c1 extends Twig_Template
{
    public function __construct(Twig_Environment $env)
    {
        parent::__construct($env);

        // line 1
        $this->parent = $this->loadTemplate("AcmeDemoBundle::layout.html.twig", "AcmeDemoBundle:Welcome:index.html.twig", 1);
        $this->blocks = array(
            'title' => array($this, 'block_title'),
            'content_header' => array($this, 'block_content_header'),
            'content' => array($this, 'block_content'),
        );
    }

    protected function doGetParent(array $context)
    {
        return "AcmeDemoBundle::layout.html.twig";
    }

    protected function doDisplay(array $context, array $blocks = array())
    {
        $this->parent->display($context, array_merge($this->blocks, $blocks));
    }

    // line 3
    public function block_title($context, array $blocks = array())
    {
        echo "Symfony - Welcome";
    }

    // line 5
    public function block_content_header($context, array $blocks = array())
    {
        echo "";
    }

    // line 7
    public function block_content($context, array $blocks = array())
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        // line 8
        echo "    ";
        $context["version"] = ((twig_constant("Symfony\\Component\\HttpKernel\\Kernel::MAJOR_VERSION") . ".") . twig_constant("Symfony\\Component\\HttpKernel\\Kernel::MINOR_VERSION"));
        // line 9
        echo "

Welcome!

Congratulations! You have successfully installed a new Symfony application.

                env, $this->env->getExtension('Symfony\Bundle\TwigBundle\Extension\AssetsExtension')->getAssetUrl("bundles/acmedemo/images/welcome-quick-tour.gif"), "html", null, true);
        echo "\" alt=\"Quick tour\" />

            env, ($context["version"] ?? $this->getContext($context, "version")), "html", null, true);
        echo "/quick_tour/index.html\" class=\"sf-button sf-button-selected\">

                        Read the Quick Tour

        ";
        // line 27
        if (($this->getAttribute(($context["app"] ?? $this->getContext($context, "app")), "environment", array()) == "dev")) {
            // line 28
            echo "

                    env, $this->env->getExtension('Symfony\Bundle\TwigBundle\Extension\AssetsExtension')->getAssetUrl("bundles/acmedemo/images/welcome-configure.gif"), "html", null, true);
            echo "\" alt=\"Configure your application\" />

                env->getExtension('Symfony\Bridge\Twig\Extension\RoutingExtension')->getPath("_configurator_home");
            echo "\" class=\"sf-button sf-button-selected\">

                            Configure

        ";
        }
        // line 41
        echo "

                env, $this->env->getExtension('Symfony\Bundle\TwigBundle\Extension\AssetsExtension')->getAssetUrl("bundles/acmedemo/images/welcome-demo.gif"), "html", null, true);
        echo "\" alt=\"Demo\" />

            env->getExtension('Symfony\Bridge\Twig\Extension\RoutingExtension')->getPath("_demo");
        echo "\" class=\"sf-button sf-button-selected\">

                        Run The Demo

Documentation

env, ($context["version"] ?? $this->getContext($context, "version")), "html", null, true);
        echo "/book/index.html\">The Book

env, ($context["version"] ?? $this->getContext($context, "version")), "html", null, true);
        echo "/cookbook/index.html\">The Cookbook

env, ($context["version"] ?? $this->getContext($context, "version")), "html", null, true);
        echo "/components/index.html\">The Components

env, ($context["version"] ?? $this->getContext($context, "version")), "html", null, true);
        echo "/reference/index.html\">Reference

env, ($context["version"] ?? $this->getContext($context, "version")), "html", null, true);
        echo "/glossary.html\">Glossary

Sensio

Trainings

Books

Community

IRC channel

Mailing lists

Forum

env, ($context["version"] ?? $this->getContext($context, "version")), "html", null, true);
        echo "/contributing/index.html\">Contributing

";
    }

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        return "AcmeDemoBundle:Welcome:index.html.twig";
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        return $this->getSourceContext()->getCode();
    }

    public function getSourceContext()
    {
        return new Twig_Source("{% extends 'AcmeDemoBundle::layout.html.twig' %}

{% block title %}Symfony - Welcome{% endblock %}

{% block content_header '' %}

{% block content %}
    {% set version = constant('Symfony\\\\Component\\\\HttpKernel\\\\Kernel::MAJOR_VERSION') ~ '.' ~ constant('Symfony\\\\Component\\\\HttpKernel\\\\Kernel::MINOR_VERSION')%}

Welcome!

Congratulations! You have successfully installed a new Symfony application.

                        Read the Quick Tour

        {% if app.environment == 'dev' %}

                            Configure

        {% endif %}

                        Run The Demo

Documentation

The Book

The Cookbook

The Components

Reference

Glossary

Sensio

Trainings

Books

Community

IRC channel

Mailing lists

Forum

Contributing

{% endblock %}
", "AcmeDemoBundle:Welcome:index.html.twig", "/Applications/MAMP/htdocs/bijen/src/Acme/DemoBundle/Resources/views/Welcome/index.html.twig");
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}

redpajama_set_name: RedPajamaGithub


Happy New Perth! I mean Happy New Year!
We had Floris join us for Christmas & New Year. You probably know him as he is from Amsterdam...195cm or 6 feet 5 he's hard to miss. Great to have your close friends join you at this time 'cos that's what this time is about...getting together. This pic for the pool room...trust it carries enduring memories that you can carry in your quieter moments. Happy New year Ralf. And may your aspirations for this year bloom.
From Amsterdam, which Dutch person doesn't know him. Thanks for the well wishes and obviously I trust this year will bring you much joy and fortitude as well! May it be a good one!


There are 8 Carpet Cleaning specialists in New Buildings, and last month we helped 147518 homeowners get quotes for their home improvement jobs.
post for gate needs strengthened damaged when pavement outside was tarmaced.
I want an outside tap installed from the kitchen wall where the sink taps are.
Sliding wardrobes and bespoke book shelves for my sons bedroom.


Campus town offers 612 student beds in an apartment setting and 83000 sq ft of retail shopes below offering food services and health care options. Ticket sales info tcf talks ham cram license exam computer club tables indoor flea market vendor fair speakervip registration parking. Tcnj on campus visits thank you for your interest in the college of new jersey.


text:
Q: Same key for two users The problem
I added a new user (adolfo) to login through SSH, so I can disable root login. After creating the user, I copied the public key from /root/.ssh/authorized_keys to /home/adolfo/.ssh/authorized_keys because I want to keep using the same key. I guess this is all right. However, if I try to login with ssh adolfo@<ip-address>, I get the error Permission denied (publickey).
Attempts to solve
I have tried following this answer but it didn't work. Though the answer advises to run chmod 644 on the authorized_keys file, I also tried chmod 600 (which was advised somewhere else). Unfortunately, it didn't make any difference.
Context
Currently, the relevant file permissions are:
$ ls -ld / /home /home/adolfo /home/adolfo/.ssh /home/adolfo/.ssh/authorized_keys
drwxr-xr-x 23 root   root   4096 Mar  8 16:45 /
drwxr-xr-x  3 root   root   4096 Mar  7 17:05 /home
drwxr-xr-x  6 adolfo adolfo 4096 Mar  7 17:49 /home/adolfo
drwx------  2 adolfo adolfo 4096 Mar  7 17:09 /home/adolfo/.ssh
-rw-------  1 adolfo adolfo  408 Mar  7 17:09 /home/adolfo/.ssh/authorized_keys

And my /etc/ssh/sshd_config:
Port 22
Protocol 2
HostKey /etc/ssh/ssh_host_rsa_key
HostKey /etc/ssh/ssh_host_dsa_key
HostKey /etc/ssh/ssh_host_ecdsa_key
HostKey /etc/ssh/ssh_host_ed25519_key
UsePrivilegeSeparation yes
KeyRegenerationInterval 3600
ServerKeyBits 1024
SyslogFacility AUTH
LogLevel INFO
LoginGraceTime 120
PermitRootLogin yes
StrictModes yes
RSAAuthentication yes
PubkeyAuthentication yes
IgnoreRhosts yes
RhostsRSAAuthentication no
HostbasedAuthentication no
PermitEmptyPasswords no
ChallengeResponseAuthentication no
PasswordAuthentication no
X11Forwarding yes
X11DisplayOffset 10
PrintMotd no
PrintLastLog yes
TCPKeepAlive yes
AcceptEnv LANG LC_*
Subsystem sftp /usr/lib/openssh/sftp-server
UsePAM no

Output of ssh -vvv adolfo@<ip-address>:
OpenSSH_7.2p2 Ubuntu-4ubuntu2.2, OpenSSL 1.0.2g  1 Mar 2016
debug1: Reading configuration data /etc/ssh/ssh_config
debug1: /etc/ssh/ssh_config line 19: Applying options for *
debug2: resolving "thread-safe.nl" port 22
debug2: ssh_connect_direct: needpriv 0
debug1: Connecting to thread-safe.nl [94.130.181.37] port 22.
debug1: Connection established.
debug1: identity file /home/aochagavia/.ssh/id_rsa type 1
debug1: key_load_public: No such file or directory
debug1: identity file /home/aochagavia/.ssh/id_rsa-cert type -1
debug1: key_load_public: No such file or directory
debug1: identity file /home/aochagavia/.ssh/id_dsa type -1
debug1: key_load_public: No such file or directory
debug1: identity file /home/aochagavia/.ssh/id_dsa-cert type -1
debug1: key_load_public: No such file or directory
debug1: identity file /home/aochagavia/.ssh/id_ecdsa type -1
debug1: key_load_public: No such file or directory
debug1: identity file /home/aochagavia/.ssh/id_ecdsa-cert type -1
debug1: key_load_public: No such file or directory
debug1: identity file /home/aochagavia/.ssh/id_ed25519 type -1
debug1: key_load_public: No such file or directory
debug1: identity file /home/aochagavia/.ssh/id_ed25519-cert type -1
debug1: Enabling compatibility mode for protocol 2.0
debug1: Local version string SSH-2.0-OpenSSH_7.2p2 Ubuntu-4ubuntu2.2
debug1: Remote protocol version 2.0, remote software version OpenSSH_7.2p2 Ubuntu-4ubuntu2.4
debug1: match: OpenSSH_7.2p2 Ubuntu-4ubuntu2.4 pat OpenSSH* compat 0x04000000
debug2: fd 3 setting O_NONBLOCK
debug1: Authenticating to thread-safe.nl:22 as 'adolfo'
debug3: hostkeys_foreach: reading file "/home/aochagavia/.ssh/known_hosts"
debug3: record_hostkey: found key type ECDSA in file /home/aochagavia/.ssh/known_hosts:5
debug3: load_hostkeys: loaded 1 keys from thread-safe.nl
debug3: order_hostkeyalgs: prefer hostkeyalgs: ecdsa-sha2-nistp256-cert-v01@openssh.com,ecdsa-sha2-nistp384-cert-v01@openssh.com,ecdsa-sha2-nistp521-cert-v01@openssh.com,ecdsa-sha2-nistp256,ecdsa-sha2-nistp384,ecdsa-sha2-nistp521
debug3: send packet: type 20
debug1: SSH2_MSG_KEXINIT sent
debug3: receive packet: type 20
debug1: SSH2_MSG_KEXINIT received
debug2: local client KEXINIT proposal
debug2: KEX algorithms: curve25519-sha256@libssh.org,ecdh-sha2-nistp256,ecdh-sha2-nistp384,ecdh-sha2-nistp521,diffie-hellman-group-exchange-sha256,diffie-hellman-group-exchange-sha1,diffie-hellman-group14-sha1,ext-info-c
debug2: host key algorithms: ecdsa-sha2-nistp256-cert-v01@openssh.com,ecdsa-sha2-nistp384-cert-v01@openssh.com,ecdsa-sha2-nistp521-cert-v01@openssh.com,ecdsa-sha2-nistp256,ecdsa-sha2-nistp384,ecdsa-sha2-nistp521,ssh-ed25519-cert-v01@openssh.com,ssh-rsa-cert-v01@openssh.com,ssh-ed25519,rsa-sha2-512,rsa-sha2-256,ssh-rsa
debug2: ciphers ctos: chacha20-poly1305@openssh.com,aes128-ctr,aes192-ctr,aes256-ctr,aes128-gcm@openssh.com,aes256-gcm@openssh.com,aes128-cbc,aes192-cbc,aes256-cbc,3des-cbc
debug2: ciphers stoc: chacha20-poly1305@openssh.com,aes128-ctr,aes192-ctr,aes256-ctr,aes128-gcm@openssh.com,aes256-gcm@openssh.com,aes128-cbc,aes192-cbc,aes256-cbc,3des-cbc
debug2: MACs ctos: umac-64-etm@openssh.com,umac-128-etm@openssh.com,hmac-sha2-256-etm@openssh.com,hmac-sha2-512-etm@openssh.com,hmac-sha1-etm@openssh.com,umac-64@openssh.com,umac-128@openssh.com,hmac-sha2-256,hmac-sha2-512,hmac-sha1
debug2: MACs stoc: umac-64-etm@openssh.com,umac-128-etm@openssh.com,hmac-sha2-256-etm@openssh.com,hmac-sha2-512-etm@openssh.com,hmac-sha1-etm@openssh.com,umac-64@openssh.com,umac-128@openssh.com,hmac-sha2-256,hmac-sha2-512,hmac-sha1
debug2: compression ctos: none,zlib@openssh.com,zlib
debug2: compression stoc: none,zlib@openssh.com,zlib
debug2: languages ctos:
debug2: languages stoc:
debug2: first_kex_follows 0
debug2: reserved 0
debug2: peer server KEXINIT proposal
debug2: KEX algorithms: curve25519-sha256@libssh.org,ecdh-sha2-nistp256,ecdh-sha2-nistp384,ecdh-sha2-nistp521,diffie-hellman-group-exchange-sha256,diffie-hellman-group14-sha1
debug2: host key algorithms: ssh-rsa,rsa-sha2-512,rsa-sha2-256,ecdsa-sha2-nistp256,ssh-ed25519
debug2: ciphers ctos: chacha20-poly1305@openssh.com,aes128-ctr,aes192-ctr,aes256-ctr,aes128-gcm@openssh.com,aes256-gcm@openssh.com
debug2: ciphers stoc: chacha20-poly1305@openssh.com,aes128-ctr,aes192-ctr,aes256-ctr,aes128-gcm@openssh.com,aes256-gcm@openssh.com
debug2: MACs ctos: umac-64-etm@openssh.com,umac-128-etm@openssh.com,hmac-sha2-256-etm@openssh.com,hmac-sha2-512-etm@openssh.com,hmac-sha1-etm@openssh.com,umac-64@openssh.com,umac-128@openssh.com,hmac-sha2-256,hmac-sha2-512,hmac-sha1
debug2: MACs stoc: umac-64-etm@openssh.com,umac-128-etm@openssh.com,hmac-sha2-256-etm@openssh.com,hmac-sha2-512-etm@openssh.com,hmac-sha1-etm@openssh.com,umac-64@openssh.com,umac-128@openssh.com,hmac-sha2-256,hmac-sha2-512,hmac-sha1
debug2: compression ctos: none,zlib@openssh.com
debug2: compression stoc: none,zlib@openssh.com
debug2: languages ctos:
debug2: languages stoc:
debug2: first_kex_follows 0
debug2: reserved 0
debug1: kex: algorithm: curve25519-sha256@libssh.org
debug1: kex: host key algorithm: ecdsa-sha2-nistp256
debug1: kex: server->client cipher: chacha20-poly1305@openssh.com MAC: <implicit> compression: none
debug1: kex: client->server cipher: chacha20-poly1305@openssh.com MAC: <implicit> compression: none
debug3: send packet: type 30
debug1: expecting SSH2_MSG_KEX_ECDH_REPLY
debug3: receive packet: type 31
debug1: Server host key: ecdsa-sha2-nistp256 SHA256:yghdaf4BIopOULvK2IipaFE6y5wVORoAXV3I6aEB55I
debug3: hostkeys_foreach: reading file "/home/aochagavia/.ssh/known_hosts"
debug3: record_hostkey: found key type ECDSA in file /home/aochagavia/.ssh/known_hosts:5
debug3: load_hostkeys: loaded 1 keys from thread-safe.nl
debug3: hostkeys_foreach: reading file "/home/aochagavia/.ssh/known_hosts"
debug3: record_hostkey: found key type ECDSA in file /home/aochagavia/.ssh/known_hosts:1
debug3: record_hostkey: found key type RSA in file /home/aochagavia/.ssh/known_hosts:2
debug3: record_hostkey: found key type ECDSA in file /home/aochagavia/.ssh/known_hosts:3
debug3: record_hostkey: found key type ED25519 in file /home/aochagavia/.ssh/known_hosts:4
debug3: load_hostkeys: loaded 4 keys from 94.130.181.37
debug1: Host 'thread-safe.nl' is known and matches the ECDSA host key.
debug1: Found key in /home/aochagavia/.ssh/known_hosts:5
debug3: send packet: type 21
debug2: set_newkeys: mode 1
debug1: rekey after 134217728 blocks
debug1: SSH2_MSG_NEWKEYS sent
debug1: expecting SSH2_MSG_NEWKEYS
debug3: receive packet: type 21
debug2: set_newkeys: mode 0
debug1: rekey after 134217728 blocks
debug1: SSH2_MSG_NEWKEYS received
debug2: key: /home/aochagavia/.ssh/id_rsa (0x7fffd694eb40)
debug2: key: /home/aochagavia/.ssh/id_dsa ((nil))
debug2: key: /home/aochagavia/.ssh/id_ecdsa ((nil))
debug2: key: /home/aochagavia/.ssh/id_ed25519 ((nil))
debug3: send packet: type 5
debug3: receive packet: type 7
debug1: SSH2_MSG_EXT_INFO received
debug1: kex_input_ext_info: server-sig-algs=<rsa-sha2-256,rsa-sha2-512>
debug3: receive packet: type 6
debug2: service_accept: ssh-userauth
debug1: SSH2_MSG_SERVICE_ACCEPT received
debug3: send packet: type 50
debug3: receive packet: type 51
debug1: Authentications that can continue: publickey
debug3: start over, passed a different list publickey
debug3: preferred gssapi-keyex,gssapi-with-mic,publickey,keyboard-interactive,password
debug3: authmethod_lookup publickey
debug3: remaining preferred: keyboard-interactive,password
debug3: authmethod_is_enabled publickey
debug1: Next authentication method: publickey
debug1: Offering RSA public key: /home/aochagavia/.ssh/id_rsa
debug3: send_pubkey_test
debug3: send packet: type 50
debug2: we sent a publickey packet, wait for reply
debug3: receive packet: type 51
debug1: Authentications that can continue: publickey
debug1: Trying private key: /home/aochagavia/.ssh/id_dsa
debug3: no such identity: /home/aochagavia/.ssh/id_dsa: No such file or directory
debug1: Trying private key: /home/aochagavia/.ssh/id_ecdsa
debug3: no such identity: /home/aochagavia/.ssh/id_ecdsa: No such file or directory
debug1: Trying private key: /home/aochagavia/.ssh/id_ed25519
debug3: no such identity: /home/aochagavia/.ssh/id_ed25519: No such file or directory
debug2: we did not send a packet, disable method
debug1: No more authentication methods to try.
Permission denied (publickey).

A: It turns out that the adolfo user was locked for some mysterious reason. I discovered this after Kusalananda asked for the sshd log, where I found a line stating that the account was locked. Unlocking it fixed the issue.

redpajama_set_name: RedPajamaStackExchange


text:
Canada: De noodzaak om blootstellinslimieten EM straling te herzien is urgent.
woensdag, 12 mei 2010 - Categorie: Onderzoeken
Bron:The Science of Total Environ. 2010 May 5. Epub ahead of print
Exposure to electromagnetic fields (non-ionizing radiation) and its relationship with childhood leukemia: A systematic review.
Calvente I, Fernandez MF, Villalba J, Olea N, Nu�ez MI.
Laboratory of Medical Investigations, San Cecilio University Hospital, CIBER de Epidemiolog�a y Salud P�blica (CIBERESP), Spain; Department of Radiology, University of Granada, Granada, Spain.
Childhood exposure to physical contamination, including non-ionizing radiation, has been implicated in numerous diseases, raising concerns about the widespread and increasing sources of exposure to this type of radiation.
The primary objective of this review was to analyze the current state of knowledge on the association between environmental exposure to non-ionizing radiation and the risk of childhood leukemia. Scientific publications between 1979 and 2008 that include examination of this association have been reviewed using the MEDLINE/PubMed database. Studies to date have not convincingly confirmed or ruled out an association between non-ionizing radiation and the risk of childhood leukemia.
Discrepancies among the conclusions of the studies may also be influenced by confounding factors, selection bias, and misclassification. Childhood defects can result from genetic or epigenetic damage and from effects on the embryo or fetus, which may both be related to environmental exposure of the parent before conception or during the pregnancy. It is therefore critical for researchers to define a priori the type and ''window'' of exposure to be assessed. Methodological problems to be solved include the proper diagnostic classification of individuals and the estimated exposure to non-ionizing radiation, which may act through various mechanisms of action.
There appears to be an urgent need to reconsider exposure limits for low frequency and static magnetic fields, based on combined experimental and epidemiological research into the relationship between exposure to non-ionizing radiation and adverse human health effects.

redpajama_set_name: RedPajamaCommonCrawl


Some lessons are best learned the hard way. It might hurt at the time but you don't forget. Just ask Matt Cheal about lambs lettuce.
Cheal, the newly-promoted head chef at Simpsons in Edgbaston, recalls a salutary mistake in his early days with the restaurant. Simpsons was then based in Kenilworth, Warwickshire, and had already gained a Michelin star. Cheal, a young commis, was tasked with preparing the cheese course for a private function for 40 diners. It was a Saturday night, the main dining room was full and the kitchen was rammed.
Cheal was tasked by boss Andreas Antona with removing the roots from the lambs lettuce, which was being served as a garnish with the cheese.
"I completely forgot about the roots. It wasn't deliberate. I wasn't trying to interfere with the presentation of anything," says Cheal.
Cheal, now 32, recounts the story after I ask him about the worst "bollocking" of his 14-year career. If he's smiling now, sipping a cappuccino in the restaurant, it was a very different story when he started out.
What was so special about the place and the team?
When Cheal says elite, he isn't exaggerating. Antona's right-hand man was Luke Tipping, now Simpsons' executive chef director. The brigade included a promising young cook called Glynn Purnell (now a Michelin-star holder in his own right), Andy Waters (who picked up a star at Edmunds in Henley-in-Arden) and Marcus Eaves, a star man at Pied à Terre in London. A decent bunch then.
Cheal's own food education started at an early age, pot-washing at The Arden Hotel on the A45 near the National Exhibition Centre. The hotel is owned by his parents, Tony and Julie, and Cheal knew from an early age that he wanted to be a chef.
School wasn't always easy. Cheal was diagnosed with dyslexia when he was 10 and concedes he was never the most academically inclined pupil. He says he could have worked a little harder at his studies at Heart of England School in Balsall Common, but he had his heart set on a career in professional kitchens.
Like his dad, Cheal trained at University College Birmingham, taking NVQ levels 1, 2 and 3 in catering and hospitality. He worked at Simpsons while at UCB and went on a placement at Lettonie in Bath, which was firing on all cylinders – and picking up two Michelin stars – under Martin Blunos. "I just fell in love with that style and standard of food," says Cheal.
He went on to earn his stripes, progressing from commis chef to chef de partie at Simpsons and picked up the British Culinary Federation Junior Chef of the Year title in 2002. He was crowned Chef of the Year in 2010.
Today, he is married to Emma and has two young daughters – Jessica, who is six, and three-year-old Phoebe. As well as being Simpsons' head chef, Matt runs the Saturday, and sometimes Sunday, cookery school.
I have no idea where he finds the energy. We dine at Simpsons on a busy Friday night and when I chat to Cheal towards the end of service he is already planning the sauces for the next day.
He has just turned out some great plates on the eight-course tasting menu, running the show in the absence of Tipping, who is on a night off. Former head chef Adam Bennett has departed the Edgbaston stronghold and is now running The Cross at Kenilworth, which is part of Simpsons' growing empire. The fact Cheal is deemed good enough to run the Simpsons' flagship tells you a lot about the faith Antona and Tipping place in him.
Among the stand-out courses is a take on scallops and pork belly. It's a familiar pairing but this starter is given new vibrancy – and colour – with leeks and watercress. The cooking of the shellfish is spot on, a common theme throughout the meal, whether it is fish or meat. The timing is perfect.
Glistening cod is given a winter warm up with lentil dhal, cauliflower and that staple of 70s British curries – sultanas. It's a nice retro touch and works well.
An elegant tranche of chicken and duck liver parfait is as fine as I've had, sweetened with a punchy beetroot jelly and brioche. The dish is matched with one of the evening's great wine pairings – a lightly acidic 2011 Trait d'union, Domaine Jousset, from Montlouis in the Loire, made from 100% chenin blanc. I know the area because my sister lived there for a while. Happily, the wine pairing worked far better than her marriage to a French chef.
One of the joys of having the sommelier pick the wines is that you try bottles off your default radar. So it was with the 2009 Numanthia, Tinto de Toro, Castilla y Leon.
This medium-bodied, tannic Spaniard has plummy and tobacco notes that work really well with Cheal's venison, the meat finished with smokey aromas. The venison is accompanied with a haggis "bolgonese" which is basically a very good sauce, and delicious salsify.
The pastry section is in good form. A lovely pre-dessert of whippy creamy loveliness and tangy pink grapefruit is followed by a coconut panna cotta, passion fruit and pineapple.
If Cheal can cook like this, it is reasonable to ask what may lie in the future. He says he would love to have his own restaurant one day, ideally in the Solihull area, but for now everything is focused on maintaining the standards established at Simpsons. For Cheal, that means using outstanding produce to produce clear flavours that the restaurant's customers love.
"I hate over-complication. I like simplicity – just well-cooked food. You don't need to confuse a dish with too many flavours," he says.


From the moment you and your loved ones step foot through the entrance of McGregor's assisted living apartments, you know something special is about to take place. We make every effort to ensure our assisted living apartments look and feel like home.
To that end, you'll be welcomed into the McGregor facility by well-manicured grounds and a sweeping columned entryway that will beckon you to keep walking, to discover what accommodating secrets we're harboring inside.
Onward to your assisted living apartment where you'll find all the creature comforts of home and more. Wood-paneled fireplaces, Oriental rugs and overstuffed wing chairs are just some of the attentions to detail we've paid in the interior design of our assisted living apartments.
Your assisted living kitchenette is equipped with all the necessities you'll require to whip together a quick lunch or bedtime snack. A full-size refrigerator/freezer combo and stainless steel sink are built into every kitchenette, and both cupboard and counter space abound.
Your living room area is tastefully decorated with table, chair and couch so that your visitors will feel just as at home as you do and every decorative item you bring with you finds its own place to call home.
A full bath with every attention paid to safety is the pièce de résistence of your McGregor assisted living apartment. Spacious countertop, handicap accessible toilet and shower with seating ensure residents of all abilities get the most out of their new McGregor assisted living apartment.


text:
\section{Introduction} \label{sec:intro}
Over the past decades, extensive observations of the solar atmosphere from the photosphere to the corona have revealed a hemispheric preference in the dominant sign of magnetic helicity, specifically a dominance of negative (left-handed) helicity in the northern hemisphere and positive (right-handed) helicity in the southern hemisphere, independent of the solar cycle. This is the so-called hemispheric sign preference (hereafter referred to as HSP) observed in numerous magnetic structures in the Sun. For example, a majority of sunspot penumbral fibrils in the northern/southern hemisphere show counterclockwise/clockwise rotations from outside to inside \citep{1927Natur.119..708H,1941ApJ....93...24R,1987SoPh..107..221D,2003AdSpR..32.1867P}. Solar prominences in the northern/southern hemisphere tend to be composed of dextral/sinistral channels with right-bearing/left-bearing barbs \citep{1994ASIC..433..303M,2003ApJ...595..500P,2009ApJ...692..104L,2017ApJ...835...94O}; this tendency is found in all cases of prominences and filaments: active-region, intermediate, and quiescent, with different degrees of compliance. Bright coronal loops displaying a distinct ``S-shape'' (called sigmoids) show their hemispheric preference in their shape as observed in (for example) soft X-ray emission, i.e., an inverse/forward S-shape in the northern/southern hemisphere \citep{1996ApJ...464L.199R,1999GeoRL..26..627C,2014SoPh..289.3297S}. This HSP is also found in strong-field plage and sunspot regions, as well as in quiet-Sun network regions, by means of the force-free-field parameter $\alpha$ and the vertical component of current helicity density calculated from photospheric vector magnetograms \citep{1995ApJ...440L.109P,1999ApJ...519..876Z,2001ASPC..236..423P,2013MNRAS.433.1648G,2013ApJ...772...52G,2015PASJ...67....6O}. Furthermore, near-Earth {\it in situ} observations of interplanetary coronal mass ejections (ICMEs) show that the handedness of twisted magnetic field lines in ICMEs is well matched with that estimated in their solar source ARs \citep{2013SoPh..284..105C}, exhibiting the relevant HSP.

Several physical processes have been proposed to explain the observed HSP in these solar magnetic structures \citep[refer to a review by][and references therein]{2002ApJ...573..445B}. The proposed processes are thought to play a crucial role in the generation of twist on magnetic flux tubes at the base of the convection zone, during their buoyant rise through the bulk of the convection zone, and by their footpoint motions in the photosphere, such as: (1) differential rotation \citep{1990SoPh..125..219S,2000JGR...10510481B,2000ApJ...539..944D,2002SoPh..207...87D}, (2) Coriolis force \citep{1985ApJ...291..300G,1997ApJ...488..443L,2013ApJ...775L..46W}, (3) $\alpha$-effect involved in turbulent dynamo models \citep{1996GeoRL..23.2649R,1996PhRvE..53.1283S,1999GMS...111...75G,2001ApJ...559..428D,2013ApJ...768...46P}, (4) helical turbulent convection \citep[called $\Sigma$-effect;][]{1998ApJ...507..417L}, and (5) local photospheric flows associated with magnetic flux cancellation and reconnection \citep{1989ApJ...343..971V,1994ApJ...427..459P,1999ApJ...515..435L,1999GMS...111..213V}. As discussed in \citet{2002ApJ...573..445B}, some of the aforementioned processes need not be mutually exclusive but may simultaneously operate in producing twist on flux tubes through the layers from the deep convection zone to the photosphere. As a result, the degree of the HSP may be either strengthened or weakened by multiple combinations of the processes acting on rising flux tubes. However, the relative importance of these different processes responsible for the HSP is still under debate. It is also not clear what causes variations in the strength of the HSP, which were observed, for example, in different phases of a solar cycle \citep{2005PASJ...57..481H,2019ApJ...882...80G,2019ApJ...887..192K} as well as in different solar features \citep{2014SSRv..186..285P}.

Magnetic helicity is a useful, quantitative measure to diagnose the underlying physical processes that govern the HSP, in terms of twists, kinks, and inter-linkages of magnetic field lines \citep[e.g.,][]{1984JFM...147..133B,2006JPhA...39.8321B,2009AdSpR..43.1013D}. Here we estimate magnetic helicity flux across the photospheric surface of active regions (ARs) over an 8-year span of 2010 through 2017, using photospheric vector magnetic field observations by the Helioseismic and Magnetic Imager \citep[HMI,][]{2012SoPh..275..207S} onboard the Solar Dynamics Observatory \citep[SDO;][]{2012SoPh..275....3P}. Analyzing the estimated magnetic helicity flux with a large sample, we intend to (1) quantitatively investigate the HSP of magnetic helicity flux for different groups as categorized by their heliographic latitudes and phase of the solar cycle, Mount Wilson magnetic classifications, and relevant magnetic field properties, (2) investigate if there are trends in the strength of the HSP with respect to those considered categorizations, and (3) support (or not) a preferred condition and relevant mechanism for adherence to the observed HSP.

\section{Observations and Data Analysis} \label{sec:obs}
\subsection{Data Set of Active Region Vector Magnetograms} \label{subsec:obs_dataset}
In this study, we analyze a data set of HMI full-disk photospheric vector magnetograms ({\tt hmi.B\_720s}) with a spatial resolution of 1{\arcsec} (pixel size of 0.5{\arcsec}) observed at 00:36 and 00:48 TAI each day from 2010 May 1 to 2017 December 31. For the given HMI data set, we first search for automatically identified HMI AR Patches \citep[HARPs;][as recorded in the {\tt hmi.M\_720s} series]{2014SoPh..289.3483H}, each of which satisfies the following criteria: (1) the HARP boundaries are located within $\pm$60$^\circ$ in longitude from the central meridian, and (2) only a single NOAA-numbered AR with at least one sunspot visible in white-light is contained in the HARP field of view (FOV). Hereafter, we will refer to such HARPs satisfying our selection criteria as ARs. HARPs containing a single NOAA-numbered AR but without a sunspot are not considered as ARs, but are categorized instead as a distinct group, namely old-region plage. Because NOAA assigns numbers only to active regions containing sunspots, numbered regions without sunspots can uniquely be considered old, decaying active region remnants. A comparison of the HSP of magnetic helicity flux between ARs and plages is presented in the Appendix.

\begin{figure}[t!]
\centering
\includegraphics[width=0.88\textwidth]{harp_dist.eps}
\caption{Frequency distributions of 4,802 HARPs considered in this study for estimation of magnetic helicity flux, with respect to (a) heliographic longitudes, (b) heliographic latitudes, (c) Carrington longitudes, and (d) observation years of the HARPs.}
\label{fig:harp_dist}
\end{figure}

The coordinates of each identified HARP are used to construct cutout images of all three vector magnetic field components from the corresponding full-disk vector magnetic field data, using the NWRA remote-SUMS/DRMS system. Over the examined period of 2010 to 2017, consequently, we obtain a total of 4,802 co-aligned pairs of AR vector magnetograms with time separation of 12 minutes, which we consider 4,802 samples. Given the definition above, this amounts to 1,105 unique NOAA numbers. While many ARs are thus sampled repeatedly with a 24 hr cadence, we consider these samples independent because magnetic helicity flux estimates can show significant variations, including sign changes, over timescales of 24 hr and longer \citep{2008ApJ...686.1397P,2010ApJ...718...43P,2012ApJ...761..105L,2017A&A...597A.104V,2018ApJ...865..139B}. For each HARP in our data set, we examined the fraction of magnetic helicity flux measurements
that are opposite that HARP's majority sign over the observing time between the longitude limits imposed.
Upon examination, the fraction is found to be 0.17, on average, for all HARPs studied here. Such observed sign changes could be caused by difference processes such as emerging magnetic flux with an opposite sign of magnetic helicity into the corona, submerging magnetic flux into the interior that brings magnetic helicity across the surface, and photospheric flows that unwind twisted magnetic field lines. Of note, because we are sampling the HMI data at the same time each day, variations in the magnetic helicity flux are likely not due to the influence of the spacecraft orbital velocity \citep{2012ApJ...761..105L,2016ApJ...823..101S}. Figure~\ref{fig:harp_dist} shows the frequency distributions of (a--c) center coordinates, and (d) observed years of all identified HARPs at 00:36 TAI. All the co-aligned AR vector magnetogram pairs are remapped from pixel coordinates in the original CCD image plane to helioplanar coordinates (here, denoted as $B_{x}$, $B_{y}$ and $B_{z}$). The $x$-axis and $y$-axis are oriented toward solar west and north, respectively, on a plane tangent to the solar surface at a point at the center of the HARP FOV, and the $z$-axis is in the vertical direction to the $x$--$y$ plane, following \citet{1990SoPh..126...21A}.

\subsection{Estimation of Photospheric Magnetic Helicity Flux} \label{subsec:obs_dhdt}
Photospheric plasma velocity fields (i.e., $v_{x}$, $v_{y}$ and $v_{z}$) in ARs are derived from the co-aligned pairs of $B_{x}$, $B_{y}$ and $B_{z}$ images at 12-minute separation with the Differential Affine Velocity Estimator for Vector Magnetograms \citep[DAVE4VM;][]{2008ApJ...683.1134S}.
The apodization window size used in DAVE4VM is set to 13\,pixels, based on the same evaluation test performed by \citet{2008ApJ...683.1134S}, but for the pairs of HMI $B_{x}$, $B_{y}$ and $B_{z}$ images in our case.

With the AR photospheric magnetic and velocity fields, we calculate the net magnetic helicity transfer rate $dH/dt$, also known as magnetic helicity flux, across the entire photospheric surface $S$ (i.e., the HARP FOV) of each AR
\begin{equation}
\frac{dH}{dt} = \int_{S} G_{\theta} (\textit{\textbf{x}}) \, dS, \label{eq:dhdt}
\end{equation}
where $G_{\theta}(\textit{\textbf{x}})$ is a photospheric surface density of magnetic helicity flux given in \citet{2005A&A...439.1191P} as
\begin{equation}
G_{\theta} (\textit{\textbf{x}}) = -{\frac{B_{z}}{2\pi}} \int_{S^\prime} \frac{\hat{\textit{\textbf{z}}} \cdot \left((\textit{\textbf{x}}-\textit{\textbf{x}}^\prime) \times (\textit{\textbf{u}}-\textit{\textbf{u}}^\prime)\right)} {{|\textit{\textbf{x}}-\textit{\textbf{x}}^\prime|^2}} B^\prime_{z} \, dS^\prime.
\label{eq:g_theta}
\end{equation}
As described in \citet{2003SoPh..215..203D}, here the photospheric flux transport velocity $\textit{\textbf{u}}$ is the horizontal velocity of photospheric footpoints of magnetic field lines defined as
\begin{equation}
\textit{\textbf{u}} = \textit{\textbf{v}}_{h} - \frac{v_{z}}{B_{z}}\textit{\textbf{B}}_{h},
\label{eq:footpoint_vel}
\end{equation}
where the subscript ``$h$'' represents the horizontal components of photospheric vector fields. It should be noted that the surface integrals in Equations~(\ref{eq:dhdt}) and~(\ref{eq:g_theta}) are carried out only for high-confidence pixels (as indicated by a value of 90 in the {\tt conf\_disambig.fits} segment; see \citep{2014SoPh..289.3483H}). Throughout this paper for notational simplicity, magnetic helicity refers to gauge-invariant relative magnetic helicity \citep{1984JFM...147..133B,1985CoPPC..9..111} with the specific choice of the Coulomb gauge for the vector potential of the potential field. $dH/dt$ reflects only magnetic helicity flux across the photosphere for a region of interest, such as would be caused by magnetic helicity transport due to emerging/submerging twisted magnetic flux tubes or photospheric footpoint motions. The estimated $dH/dt$ in this study therefore does not necessarily represent the HSP of the overall magnetic helicity content in the full coronal volume above said region of interest.

\begin{figure}[t!]
\centering
\includegraphics[width=0.92\textwidth]{dhdt_error.eps}
\caption{Results from Monte Carlo simulations to determine the uncertainty in the calculation of $dH/dt$ with a sample of 39 unique NOAA-numbered ARs. Scatter plots of (a) the standard deviation ($\sigma_{dH/dt}$) and (b) the ratio of $\sigma_{dH/dt}$ to the absolute value of the mean ($|\!\!<\!\!dH/dt\!\!>\!\!|$) are shown as a function of $|\!\!<\!\!dH/dt\!\!>\!\!|$. The sold line in each panel represents the least squares regression line. In panel (a), the dotted line indicates the $x$\,$=$\,$y$ line.}
\label{fig:dhdt_error}
\end{figure}

\subsection{Uncertainties in Magnetic Helicity Flux Estimates} \label{subsec:obs_uncertainty}
The uncertainty in the calculation of $dH/dt$ is estimated from a Monte Carlo simulation as follows. (1) To each data point in a co-aligned pair of 12-minute-separated $B_{x}$, $B_{y}$ and $B_{z}$ maps of a given AR, we add a noise value randomly taken from a Gaussian distribution with the standard deviation corresponding to the uncertainty in each component of the magnetic field vector as propagated from the reported ``{\tt error}'' segments provided from the Milne-Eddington inversion of the HMI Stokes profiles \citep{2014SoPh..289.3483H}, assuming the disambiguation is perfect. (2) $v_{x}$, $v_{y}$ and $v_{z}$ are determined, applying the DAVE4VM method to the pair of $B_{x}$, $B_{y}$ and $B_{z}$ with random Gaussian noise added. (3) $dH/dt$ is estimated from Equations~(\ref{eq:dhdt})--(\ref{eq:footpoint_vel}). (4) The procedure of (1) to (3) is repeated 100 times so that the mean ($<\!\!dH/dt\!\!>$) and standard deviation ($\sigma_{dH/dt}$) values of $dH/dt$ are determined. Figure~\ref{fig:dhdt_error} presents the Monte Carlo simulation results for 39 different NOAA-numbered ARs. The ratio of $\sigma_{dH/dt}$ to the absolute value of the mean $|\!\!<\!\!dH/dt\!\!>\!\!|$ is considered here as the relative error in the magnitude of the estimated $dH/dt$. We find that the smaller the value of $|\!\!<\!\!dH/dt\!\!>\!\!|$, the larger the relative error. It is found that as $|\!\!<\!\!dH/dt\!\!>\!\!|$ decreases to $10^{31}$\,Mx$^{2}$\,s$^{-1}$, the relative error becomes close to unity, in which case there may be considerable uncertainties associated with the determination of the sign of $dH/dt$. Note that only $\sim$0.8\% of our examined AR vector magnetogram data set (i.e., 40 out of 4,802) show $|dH/dt|$\,$\leq$\,$10^{31}$\,Mx$^{2}$\,s$^{-1}$ so that the results from this HSP study of $dH/dt$ are thought to be minimally affected by uncertainties in magnetic helicity flux estimates.

\section{Results} \label{sec:results}
\subsection{Dependence of the Hemispheric Helicity Sign Preference} \label{subsec:results_hsp}

\begin{figure}[t!]
\centering
\includegraphics[width=0.8\textwidth]{hist_dhdt.eps}
\caption{Relative frequency distribution of $dH/dt$ values for ARs in the northern (blue) and southern hemispheres (red), respectively.}
\label{fig:hist_dhdt}
\end{figure}

\begin{figure}[t!]
\centering
\includegraphics[width=0.78\textwidth]{hsp_1_ar.eps}
\caption{Fraction of ARs in the northern (left column) and southern (right column) hemispheres, respectively, following the HSP of $dH/dt$, as a function of (a) date, (b) heliographic latitude, and (c) $|dH/dt|$. Error bars represent Poisson uncertainties in the HSP, each of which is calculated as $1/\sqrt{N}$, where $N$ is the total number of SHARP images pairs in each bin.}
\label{fig:hsp_1_ar}
\end{figure}

\begin{figure}[t!]
\centering
\includegraphics[width=0.78\textwidth]{hsp_2_ar.eps}
\caption{Same as Figure~\ref{fig:hsp_1_ar}, but for the HSP of $dH/dt$ as a function of (a) the total unsigned magnetic flux $\Phi$, (b) the average force-free parameter $<\!\!\alpha\!\!>$, and (c) the average flow speed $<\!\!|v|\!\!>$ across the entire photospheric surface $S$ of the given AR.}
\label{fig:hsp_2_ar}
\end{figure}

With $dH/dt$ determined for each of 4,802 photospheric vector magnetogram pairs, we examine the degree and characteristics of the HSP over the 8-year period from 2010 to 2017 of solar cycle 24. Figure~\ref{fig:hist_dhdt} shows the relative frequency distribution of $dH/dt$ values for ARs in the northern (blue curve) and southern hemispheres (red curve), respectively. The $dH/dt$ distribution for the AR samples in the northern hemisphere exhibits a negative skewness with the mean of $-0.24\times10^{37}$\,Mx$^{2}$\,s$^{-1}$, while samples in the southern hemisphere show a positive skewness with the mean of $0.26\times10^{37}$\,Mx$^{2}$\,s$^{-1}$.
For all of the AR samples, the degree of the HSP of $dH/dt$ is found to be 63$\pm$0.1\% of 2,530 in the northern hemisphere and 65$\pm$0.1\% of 2,272 in the southern hemisphere, which is within the range reported in previous studies \citep[e.g.,][]{1998ApJ...507..417L,2001ApJ...549L.261P,2005PASJ...57..481H,2006ApJ...646L..85Z,2014ApJ...783L...1L}. There is also a weak tendency for ARs with larger values of $|dH/dt|$ to show a higher degree of the HSP: for example, 69$\pm$0.2\% and 70$\pm$0.2\% for a subset of ARs with $|dH/dt|$\,$>$\,$10^{37}$\,Mx$^{2}$\,s$^{-1}$ in the northern and southern hemispheres, respectively. Moreover, we divided all ARs into three subgroups as to their Mount Wilson classifications (specifically the alpha, beta, and other complex classes), and include the distributions of $dH/dt$ values for each. No significant difference is however found in the distributions between the AR subgroups. Note that by analyzing the force-free parameter $\alpha$ in 148 ARs, \citet{2014ApJ...783L...1L} found a weak tendency for the alpha- or beta-class ARs to have a higher HSP than the other complex-class ARs; however, the differences in the HSP of $\alpha$ between the different Mount Wilson classifications was not statistically significant due to the small sample size.

We now investigate any dependence of the HSP of $dH/dt$ on broad properties of ARs. Figure~\ref{fig:hsp_1_ar} shows the fraction of ARs in the northern and southern hemispheres, respectively, that follow the HSP, as a function of (a) date (as a proxy for solar cycle phase, assuming a rough 2010 start date), (b) heliographic latitude, and (c) $|dH/dt|$. The HSP tends to gradually increase from $\sim$50\,--\,60\% up to $\sim$70\,--\,80\% for AR samples appearing at an earlier date of the examined period, or a higher latitude. This implies that ARs in the inclining phase of solar cycle 24 are more likely to comply with the HSP than those in the declining phase. The observed dependence of the HSP on the solar cycle phase was also found by other studies \citep[e.g.,][]{2005PASJ...57..481H,2013MNRAS.433.1648G,2014ApJ...783L...1L,2019ApJ...877L..36P} in which the HSP was evaluated with different measures of magnetic twist such as the force-free parameter $\alpha$ and vertical current helicity density. In the case of \citet{2005PASJ...57..481H}, we draw particular attention to the years categorized as activity minimum and maximum periods of solar cycles 21--23 in their study, and found that the activity minimum period mostly consists of the late declining phase of the solar cycles (i.e., several years after the sunspot maximum), while the maximum period contains the early inclining phase. We note that our study quantitatively shows the HSP of $dH/dt$ as a function of date and latitude, for the first time, from the inclining to declining phases of solar cycle 24. In addition, a weak tendency is found that ARs with larger values of $|dH/dt|$ have a higher HSP.

The HSP dependence is also examined in the context of other physical properties of AR photospheric magnetic and velocity fields. Figure~\ref{fig:hsp_2_ar} shows the HSP of $dH/dt$, as a function of (a) the total unsigned magnetic flux $\Phi$, (b) the average force-free parameter $<\!\!\alpha\!\!>$, and (c) the average flow speed $<\!\!|v|\!\!>$ through the entire HARP FOV, where $|v|=\sqrt{v_{x}^2+v_{y}^2+v_{z}^2}$. Note that $<\!\!\alpha\!\!>$ and $<\!\!|v|\!\!>$ are calculated only from the same high-confidence pixels with {\tt conf\_disambig}\,$=$\,90 as used in calculating $dH/dt$. We find a higher HSP for ARs with larger values of $\Phi$ or $<\!\!|v|\!\!>$. A similar increasing trend of the HSP with stronger magnetic fields has been reported by \citet{2020SoPh..295...106} in which they examined $\alpha$, vertical current helicity density, and kinetic helicity density parameters from measurements of photospheric magnetic fields and near surface sub-photospheric flow fields in 189 ARs observed during the descending phase of the solar cycle 23. Investigating current helicity density derived from synoptic maps of the photospheric vector magnetic field, \citet{2006ApJ...646L..85Z} and \citet{2013ApJ...772...52G} also reported that strong-field ($B_{z}$\,$>$\,1000 G) regions show a higher degree of the HSP as compared to weak-field (100 G\,$<$\,$B_{z}$\,$<$\,500 G) regions. Finally, as expected, the HSP compliance of $dH/dt$ is lower for ARs for which the sign of $<\!\!\alpha\!\!>$ is positive/negative in the northern/southern hemisphere, (i.e., opposite to that expected from the HSP, and confirming the correlation between $dH/dt$ and $<\!\!\alpha\!\!>$).

\subsection{Interpretations} \label{subsec:results_interpret}
We offer some interpretations of our observational findings on the HSP dependence of $dH/dt$ with respect to various properties of ARs. Before interpreting the HSP dependence, we remind the reader that solar dynamo models need to reproduce these observed HSP dependencies as well as the degree of overall conforming to the HSP at the $\sim$60\% level as shown in Figure~\ref{fig:hist_dhdt}.

First, an enhancement of the HSP can be made by the Coriolis force (including the small-scale $\Sigma$-effect) acting on a buoyantly rising and expanding flux tube through the turbulent convection zone, as it generates the twist of magnetic field lines inside the flux tube which has a sign agreeing with the HSP. The twist will be more effectively induced by the Coriolis force in cases where a flux tube (1) rises through the bulk of the convection zone at a higher latitude; (2) has larger magnetic flux so that both the rising speed and expansion of the flux tube are faster due to larger magnetic buoyancy and pressure. This scenario of the HSP enhancement is in good agreement with our observational findings that the HSP of $dH/dt$ is positively correlated with heliographic latitude, $\Phi$, and $<\!\!|v|\!\!>$, respectively. On the other hand, the Coriolis force acting on the photospheric footpoints of an emerged flux tube will produce positive/negative magnetic helicity in the northern/southern hemisphere (i.e., a negative contribution to the HSP). The observed dependencies of the HSP on heliographic latitude and $<\!\!|v|\!\!>$, however, suggest that this action of the Coriolis force may be relatively weak compared to other sources of the HSP.

Another important process that can generate and modify twist on flux tubes is differential rotation. A negative contribution to the HSP will be made in the convection zone by a shearing action of differential rotation on a rising $\Omega$-shaped flux tube with a tilt between its leading and following legs of opposite polarities. This suggests that a flux tube rising through a localized region of the convection zone with a larger degree of differential rotation may have an opposite sign of magnetic helicity as compared to the one expected from the HSP. In the global-scale three-dimensional convective dynamo simulations by \citet{2014ApJ...789...35F,2016AdSpR..58.1497F}, it is found that the presence of strong, large-scale magnetic fields at the base of the convection zone results in a more enhanced outward Reynolds stress and consequently a larger differential rotation. Moreover, the differential rotation in the convection zone is found to be larger at a higher latitude in both simulations and helioseismic observations \citep[see a review by][and references therein]{2009LRSP....6....1H}. In contrast to the above-mentioned possible ways of weakening the HSP by the differential rotation, our results, however, show an increasing trend of the HSP of $dH/dt$ with $\Phi$, as well as with latitude, which implies that the HSP may be less impacted by the differential rotation in the convection zone. Contrary to the shearing action of differential rotation in the convection zone, the photospheric differential rotation on the solar surface will lead to the enhancement of the HSP, twisting the footpoints of emerged magnetic fields and shearing a bipolar sunspot pair of an emerged $\Omega$-shaped flux tube. The observed increase of the HSP of $dH/dt$ with increasing latitude supports the scenario that the HSP is strengthened by a larger surface differential rotation observed at a higher latitude \citep{2014AJ....148..101S,2017ApJ...836...10L}.

Meanwhile, the tachocline $\alpha$-effect of flux-transport dynamos \citep[e.g.,][]{1999GMS...111...75G,2001ApJ...559..428D} at the base of the convection zone will generate a twisted flux tube of which helicity sign follows the HSP. It is shown that the relative amplitude of the tachocline $\alpha$-effect in the latitude range of $\sim$30{\degr}--50{\degr} is much larger than that at lower latitudes. Consequently, a higher HSP is expected at higher latitudes, which is supported by the observed positive correlation between the HSP of $dH/dt$ and latitude.

\section{Summary and Conclusions} \label{sec:discussion}
Magnetic helicity is a useful, quantitative measure to examine the handedness of twisted magnetic field lines observed in various magnetic structures in the solar atmosphere. In this paper we have investigated magnetic helicity flux ($dH/dt$) across the photospheric surface for 4,802 samples of 1,105 unique active regions that appeared over an 8-year period from 2010 to 2017 of solar cycle 24. Through the analysis of the AR magnetic helicity flux estimates, we found that 63\% and 65\% of the samples in the northern and southern hemispheres, respectively, follow the hemispheric sign preference (HSP): i.e., displaying predominantly the left-handed/right-handed sign of $dH/dt$ in the northern/southern hemisphere. It is also found that the HSP compliance of $dH/dt$ increases from $\sim$50\,--\,60\% up to $\sim$70\,--\,80\% in cases where the ARs (1) appeared during the inclining phase of the solar cycle, or at higher latitudes; (2) had larger values of $|dH/dt|$, the total unsigned magnetic flux, or the average plasma-flow speed; (3) displayed the same sign between the average force-free parameter and that expected from the HSP (i.e., negative/positive in the northern/southern hemisphere).

All of these observational findings lend support to the scenario that the HSP of $dH/dt$ is enhanced primarily by the Coriolis force acting on a buoyantly rising and expanding flux tube through the turbulent convection zone. In addition, the action of differential rotation on the solar surface as well as the tachocline $\alpha$-effect of flux-transport dynamos may also reinforce the HSP for ARs observed at higher latitudes. Meanwhile, the observed HSP tendencies imply that an expected weakening of the HSP by the differential rotation in the convection zone is less significant compared to the enhancement of the HSP by the Coriolis force in the convection zone, the photospheric differential rotation, and/or the tachocline $\alpha$-effect. We urge research that employs state-of-the-art solar convective dynamo simulations to explore and use as model validation the trends put forth here, in order to judge the relative input of relevant processes to helicity transport throughout the solar cycle.

\acknowledgments
The authors would like to thank an anonymous referee for constructive comments that helped clarify aspects of this paper. The authors also thank Graham Barnes, Eric Wagner, Orion Poplawski, and the NWRA/Boulder team for the development and maintenance of the SDO remote SUMS/DRMS site and analysis servers at NWRA. The data used in this work are courtesy of the NASA/SDO and the HMI science teams. This research has made extensive use of the NASA's Astrophysics Data System (ADS) as well as the computer system of the Center for Integrated Data Science (CIDAS), Institute for Space-Earth Environmental Research (ISEE), Nagoya University. This work was partially supported by MEXT/JSPS KAKENHI Grant No.~JP15H05814.
\vspace{5mm}
\facilities{SDO (HMI)}
\software{DAVE4VM \citep{2008ApJ...683.1134S}}

\input{ms.bbl}

\clearpage

\section*{Appendix: Comparison of the Hemispheric Helicity Sign Preference between Active Regions and Plage Regions} \label{sec:appendix}
\begin{figure}[t!]
\centering
\includegraphics[width=0.78\textwidth]{hsp_1_pr.eps}
\caption{Same as Figure~\ref{fig:hsp_1_ar}, but for plage areas (circles with error bars). The HSP of $dH/dt$ for ARs (red diamonds without error bars) in Figure~\ref{fig:hsp_1_ar} are also shown for comparison.}
\label{fig:hsp_1_pr}
\end{figure}

\begin{figure}[t!]
\centering
\includegraphics[width=0.78\textwidth]{hsp_2_pr.eps}
\caption{Same as ARs (red diamonds) shown in Figure~\ref{fig:hsp_2_ar}, but for plage regions (circles with error bars). The HSP of $dH/dt$ for ARs (red diamonds without error bars) in Figure~\ref{fig:hsp_2_ar} are also shown for comparison.}
\label{fig:hsp_2_pr}
\end{figure}

Plage regions are observed as bright areas in H$\alpha$ line center images without a dark sunspot in the continuum. In particular with the dataset considered here, plage regions may be assumed to be aged regions with decaying magnetic fields. In this section we investigate whether there is any difference of the HSP of $dH/dt$ between ARs and plages. For this, we first searched HARPs over the same investigated period of $\sim$8 years (i.e., 2010 May 1 to 2017 December 31), each of which contains only a single NOAA-numbered plage identified in the NOAA Solar Region Summary archive (\url{ftp://ftp.swpc.noaa.gov/pub/warehouse}). A total of 1,456 daily samples are assigned to 488 unique NOAA-identified plage areas, specifically 795 and 661 samples in the northern and southern hemispheres, respectively. Figures~\ref{fig:hsp_1_pr} and~\ref{fig:hsp_2_pr} show the HSP of $dH/dt$ for plage samples (black circles with error bars) as a function of the region properties described in Figures~\ref{fig:hsp_1_ar} and~\ref{fig:hsp_2_ar}, with the HSP of $dH/dt$ for ARs (red diamonds) also shown for reference. We find that ARs and plages exhibit similar overall trends in the strength of the HSP of $dH/dt$ with respect to the properties considered (explained in detail in Section~\ref{subsec:results_hsp}). Even though some differences are found in the HSP trends between ARs and plages (e.g., see panel (c1) of Figure~\ref{fig:hsp_2_pr} for samples with $<\!\!|v|\!\!>$ below 0.2 km/s), it should be noted that the statistical significance of such differences is limited, due to the comparatively small number of plage samples.

\end{document}

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I wanted my body of work, Curiouser and curiouser , to illustrate a simple story where a catalyst motivates the protagonist through a journey. Taking the title from Lewis Carroll's Alice in Wonderland , and influenced by my love of cartoons and picture books, I worked with a graphics tablet and digital medium to explore a human being's natural curiosity. Setting is a key feature in my work, with the character finding herself in surreal landscapes. Through the character's journey I explored the notion of curiosity, and how it leads to new experiences in the world.


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text:
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Kerala Tourism has come up with a new slogan 'Human by Nature' to gain global attention. The campaign was launched on February 18 by Mr Kadakampally Surendran, Minister for Tourism, in the presence of Ms Rani George, Secretary, Kerala Tourism, and Mr P.Bala Kiran, Director, Kerala Tourism, at a function at Lalit hotel. The screening of a 3-minute short film developed as part of the campaign was inaugurated by the celebrated classical dancer and actor Ms Shobana.
The minister said that the campaign will put Kerala Tourism on a higher pedestal in the competitive global marketplace.
Ms Rani George said that the film was both classy and touching. It showed Kerala in a wider spectrum as vibrant and welcoming, underlined by a powerful human touch. According to the director, it was a visual depiction of life in Kerala. The campaign will be conducted in Kerala Tourism's key markets, such as the USA, the UK, the Gulf countries, Germany, France, Spain, the Netherlands, Switzerland, and Belgium.


text:
Foodie Gossip
Who's Cooking
The Pie Shoppe Debuts in Hicksville
Good Eats reshmi kaur oberoi | November 9, 2016
Contractor Spiro Kitovas has constructed everything from bridges to The Metropolitan Detention Center in Brooklyn, the Fire Alarm System at Queens College and The Police Academy in College Point, but that hasn't been enough to cure his cravings for creativity. In search of a sweeter life, Kitovas opened The Pie Shoppe, a scratch bakery in Hicksville, in September.
Kitovas said his pies have a "homey connotation to them." Keeping home in mind, he used his knack for designing to create the 4,000-square-foot facility with dark wooden finishes, a redwood colored brick wall and a forest green scalloped canopy over windows that showcase pies, avant-garde layered cakes and a nifty cappuccino contraption.
The Pie Shoppe's menu is just as inviting. Everything is made on premise, including the jams and marshmallows. There are sweet pies like pumpkin, sweet potato, key lime and fruit-filled pies that are baked and served in a paper bag to keep the natural juices from evaporating. Get there early for the savory breakfast egg pies, made with bacon or sausage, cheese and housed in the customer's choice of hash browns or Panko breadcrumbs, which are served promptly until 11:30am. Hearty potpies options are also available with fillings like spinach (his mother's recipe for the traditional Greek spanakopita), braised short ribs, turkey and bourbon chicken.
There's a made-to-order cake section in an allotted space in the far corner, away from the pies and coffee bar that has its own audience. The staff will put a tray full of bits and pieces from The Pie Shoppe's mainstay cookies on the counter from time to time so guests can take a taste.
Like the guests, Kitovas loves to taste but the businessman, contractor and visionary doesn't cook. "I couldn't fry an egg to be honest with you," he confessed. "But I have dabbled in pastry and I do know the process and what we have to do to make every single item we sell." That's how he knew to weed out prospective pastry consultants and team up with award-winning pastry chef, Robert Ellinger.
Ellinger was the head chef at Port Washington's heralded Baked to Perfection, which closed down earlier this year. Kitovas attended an auction Ellinger hosted in hopes of purchasing commercial baking kitchen essentials. They got to talking and Ellinger agreed to help develop pie recipes, even funneling a few of his disciples along to Kitovas, including the cake decorator who doubles as head baker.
Kitovas plans to incorporate more of his Greek heritage into The Pie Shoppe's future plans, one of which is The Custard Pie—a hand pie that is best served hot, is surrounded by phyllo dough covered in powdered sugar and cinnamon. Kitovas asserts that this is "the best breakfast, if you like sugar," and will be one of "several products that we're going to introduce over the next several months."
He's finalizing the liquor license and will soon introduce Irish coffee, an espresso with a shot of Sambuca, and a self-proclaimed "excellent chai tea latte gin" that "you'll fall in love with if you try it once and you'll never stop drinking it."
Sipping to The End
A trio of toasts
Can You Taste It?
The sacred vino vessel gets canned


text:
DATELINE: MIDDLETON
Opening Day!
You can't eat. You can't sleep. Your head is filled with magical visions.
BY RED MULCAHY Special to Beacon Athletics — Is it Christmas Eve? No, much better than that. It's Opening Day. The visions you have aren't of sugarplums, but of an emerald green ballfield, a juicy hot dog slathered in relish, an acrobatic shortstop whirling in midair to throw out a speeding runner.
This is the day that drives a stake through the heart of winter. Nothing but sunny skies and balmy breezes ahead. And your team — whatever its woeful history — has a clean slate. This could be the year. It really could. (Just ask the 2016 Chicago Cubs.)
It should be a national holiday. In 2014, Ozzie Smith and Anheuser-Busch campaigned to make it one, but without success, at least not yet. No matter. All across the country, we'll be playing hooky from work or school to catch the opener of our favorite team — and of course it will feel that much sweeter because it isn't a holiday.
In Cincinnati, things are different. The Reds were the very first major league team, founded in 1869. To honor that, they open every season at home. Opening Day is a city holiday, and there's a lively parade. The Findlay Market Parade marches down Race Street to 5th, left past the Taft Theater and then on to the Great American Ballpark.
On Opening Day, we can count on whoever is the current chicken-winged President to throw out the first ball. And at least one celebrity to absolutely murder the National Anthem, as the crowd showers down good-natured boos and catcalls.
Expect surprises, and history to be made. In 1907, the New York Giants forfeited their game at the Polo Grounds when rowdy fans wouldn't stop pelting the field with snowballs. In 1940, Bob Feller tossed a no-hitter. In 1974, Hammerin' Hank Aaron belted his 714th career homer, tying Babe Ruth for the all-time lead.
Everyone feels the excitement of Opening Day — even the most highly paid major league ballplayers. No less an icon than Joe DiMaggio said: "You always get a special kick on Opening Day, no matter how many you go through. You look forward to it like a birthday party when you're a kid. You think something wonderful is going to happen."
Paul Zwaska of Beacon Athletics spent twelve years as head groundskeeper of the Baltimore Orioles. For him, Opening Day always brought a sense of pride as well as excitement. "We'd been working outside on the ballfield since around March 1st. We'd talk about how quiet the stadium was. And we'd begin to count the days until Camden Yards was full of fans again, looking down at our artful groundskeeping, our rake strokes and mowing patterns, the crisp chalk lines, the colorful palette of greens, reds, tan, brown and white."
Nothing can match the hoopla of a major league Opening Day, but for many of us, the most memorable Opening Day is the one that happens closer to home, when our son or daughter makes their first appearance at the Little League park, or even the weedy t-ball field down the street.
You know your kid probably has a bad case of butterflies — just like you did, thirty years before. You know that the first time up, they may whiff on three wild swings — just like you did, thirty years before. But there'll be redemption, too — a solid hit, late in the game, or a backhanded grab of a hot grounder.
Hopefully, they'll catch the baseball bug, and not abandon the sport for soccer or basketball. Because there's nothing like this game — nothing else even comes close — and Opening Day is the day we welcome it back again, with appropriate celebration, realizing just how much we've missed it.
Now, where did we put that old fielder's glove, the one with the Dick McAuliffe signature? Just in case someone clouts one into the upper deck.
Visit Beacon Athletics
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text:
Formula One drivers all wear End Racism T-shirts at season-opening Austrian Grand Prix
Posted on July 06, 2020, 3:02 pm
Issued on: 05/07/2020 – 20:23Modified: 05/07/2020 – 20:23
Valtteri Bottas kneeled holding the winners trophy at Formula One's season-opening Austrian Grand Prix on Sunday, where the podium trio held up a black T-shirt with "End Racism" written on it.
That message was said before the race, too, when all drivers wore that T-shirt. World champion Lewis Hamilton, the only black driver in F1, had Black Lives Matter on the front and End Racism on the back of his.
But six did not join Hamilton and 13 others in taking the knee: Kimi Raikkonen, Max Verstappen, Daniil Kvyat, Antonio Giovinazzi, Carlos Sainz Jr. and Charles Leclerc — who finished in second place.
Hamilton, who knelt alongside Sebastian Vettel, at one point bowed his head pensively while Kvyat pointed to the anti-racism message on his T-shirt.
Hamilton has spoken widely about racism in recent weeks following the death in Minneapolis of George Floyd — a handcuffed and unarmed Black man — after a police officer pressed his knee on Floyds neck for nearly nine minutes in May. Hamilton attended a Black Lives Matter march in London and is setting up a commission to increase diversity in motorsport.
Soccer players on fields in England and Germany have taken the knee together simultaneously before games in support of the Black Lives Matter movement, and F1 drivers discussed what they should do during a drivers briefing on Friday evening.
Leclerc and Verstappen wrote on Twitter before the race why they chose not to kneel.
"I believe that what matters are facts and behaviours in our daily life rather than formal gestures that could be seen as controversial in some countries," Leclerc said. "I will not take the knee but this does not mean at all that I am less committed than others in the fight against racism."
Verstappen explained his choice.
"I am very committed to equality and the fight against racism. But I believe everyone has the right to express themselves at a time and in a way that suits them," the Dutch driver said. "I will not take the knee today but respectRead More – Source
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